Results from cosmological hydrodynamical simulations on the chemical enrichment of cosmic structures, from galaxies to groups and clusters, can be very sensitive to the specific assumptions on the IMF or of stellar yields.
In particular, these can affect the normalization of metallicity profiles and the value of global abundances.
Changes in the underlying IMF functional form, affect directly the final ICM metallicity and abundance ratio profiles, for instance, due to different relative amounts of low- and high-mass stars [1]}, [2]}, [3]}.
The yield tables are also an important source of uncertainty [4]} in the predicted integrated level of enrichment, as well as the supernova rates .
More importantly, the complex interplay with other gas thermal and dynamical processes treated in the simulations, such as energetic feedback or merging processes,
can substantially impact the spatial distribution of metals and therefore the gradients of the radial profiles, as further discussed in §REF  (see also §REF ).
